Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.209...93s&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 209, July 1, 1984, p. 93-109.
Astronomy and Astrophysics
Astronomy
191
Galactic Rotation, Galactic Structure, Spiral Galaxies, Stellar Motions, Angular Velocity, Astronomical Models, Collision Parameters, Density Distribution
Scientific paper
The response of a gaseous disk to rotating stellar bars of various strengths and pattern speeds is studied using a particle scheme in which the gas 'clouds' move as free particles except where their trajectories cross. Inelastic collisions are introduced to treat the shocks which occur at these locations. The arm-to-interarm density contrast and the pitch angle of the induced spiral arms both increase with increasing bar strength. A widening region exists in which stable periodic orbits are difficult to find until the region encompasses the whole annulus between corotation (CR) and the outer Lindblad resonance. Stars moving in quasi-stochastic orbits originating in this region form an exponential tail in the surface density profile of the stellar disk. As the pattern speed is lowered, more structure appears inside CR which may give rise to the inner rings found near the ends of bars in SB systems.
No associations
LandOfFree
How bar strength and pattern speed affect galactic spiral structure does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with How bar strength and pattern speed affect galactic spiral structure, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and How bar strength and pattern speed affect galactic spiral structure will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1707904